Model chemistry course unit 2
|Unit Summary |
|How can we explain the origin of Earth's chemistry? |
|In this unit of study, energy and matter are studied further by investigating the processes of nuclear fusion and fission that govern the formation, evolution, and workings of the solar system in the |
|universe. Students examine the processes governing the formation, evolution, and workings of the solar system and universe. Some concepts studied are fundamental to science, such as understanding how the|
|matter of our world formed during the Big Bang and within the cores of stars. Others concepts are practical, such as understanding how short-term changes in the behavior of our sun directly affect |
|humans. Engineering and technology play a large role here in obtaining and analyzing the data that support the theories of the formation of the solar system and universe. The crosscutting concepts of |
|patterns; scale, proportion, and quantity; energy and matter; and interdependence of science, engineering, and technology are called out as organizing concepts for these disciplinary core ideas. Students|
|demonstrate proficiency in developing and using models; using mathematical and computational thinking, constructing explanations; and obtaining, evaluating, and communicating information; and to use |
|these practices to demonstrate understanding of the core ideas. |
|This unit is based on HS-PS1-8, HS-ESS1-3, HS-ESS1-1, HS-ESS1-2, and HS-ESS1-6. [Note: The disciplinary core ideas, science and engineering practices, and crosscutting concepts can be taught in either |
|this course or in a high school chemistry course. If this unit is included in the Capstone course, it becomes an Earth and Space science course, rather than an environmental science course.] |
|Student Learning Objectives |
|Develop models to illustrate the changes in the composition of the nucleus of the atom and the energy released during the processes of fission, fusion, and radioactive decay. [Clarification Statement: |
|Emphasis is on simple qualitative models, such as pictures or diagrams, and on the scale of energy released in nuclear processes relative to other kinds of transformations.] [Assessment Boundary: |
|Assessment does not include quantitative calculation of energy released. Assessment is limited to alpha, beta, and gamma radioactive decays.] (HS-PS1-8) |
|Communicate scientific ideas about the way stars, over their life cycle, produce elements. [Clarification Statement: Emphasis is on the way nucleosynthesis, and therefore the different elements created, |
|varies as a function of the mass of a star and the stage of its lifetime.] [Assessment Boundary: Details of the many different nucleosynthesis pathways for stars of differing masses are not assessed.] |
|(HS-ESS1-3) |
|Develop a model based on evidence to illustrate the life span of the sun and the role of nuclear fusion in the sun’s core to release energy that eventually reaches Earth in the form of radiation. |
|[Clarification Statement: Emphasis is on the energy transfer mechanisms that allow energy from nuclear fusion in the sun’s core to reach Earth. Examples of evidence for the model include observations of |
|the masses and lifetimes of other stars, as well as the ways that the sun’s radiation varies due to sudden solar flares (“space weather”), the 11-year sunspot cycle, and non-cyclic variations over |
|centuries.] [Assessment Boundary: Assessment does not include details of the atomic and subatomic processes involved with the sun’s nuclear fusion.] (HS-ESS1-1) |
|Construct an explanation of the Big Bang theory based on astronomical evidence of light spectra, motion of distant galaxies, and composition of matter in the universe. [Clarification Statement: Emphasis |
|is on the astronomical evidence of the red shift of light from galaxies as an indication that the universe is currently expanding, the cosmic microwave background as the remnant radiation from the Big |
|Bang, and the observed composition of ordinary matter of the universe, primarily found in stars and interstellar gases (from the spectra of electromagnetic radiation from stars), which matches that |
|predicted by the Big Bang theory (3/4 hydrogen and 1/4 helium).] (HS-ESS1-2) |
|Apply scientific reasoning and evidence from ancient Earth materials, meteorites, and other planetary surfaces to construct an account of Earth’s formation and early history. [Clarification Statement: |
|Emphasis is on using available evidence within the solar system to reconstruct the early history of Earth, which formed along with the rest of the solar system 4.6 billion years ago. Examples of evidence|
|include the absolute ages of ancient materials (obtained by radiometric dating of meteorites, moon rocks, and Earth’s oldest minerals), the sizes and compositions of solar system objects, and the impact |
|cratering record of planetary surfaces.] (HS-ESS1-6) |
|Quick Links |
|Unit Sequence p. 2 |
|What it Looks Like in the Classroom p. 5 |
|Connecting with ELA/Literacy and Math p. 6 |
|Modifications p. 7 |
|Research on Learning p. 7 |
|Prior Learning p. 8 |
|Connections to Other Courses p. 9 |
|Sample of Open Education Resources p. 10 |
|Appendix A: NGSS and Foundations p. 11 |
| |
|Part A: Why is fusion considered the Holy Grail for the production of electricity? |
|Why aren’t all forms of radiation harmful to living things? |
|Concepts |Formative Assessment |
|Nuclear processes, including fusion, fission, and radioactive decay of unstable nuclei, involve |Students who understand the concepts are able to: |
|release or absorption of energy. |Develop models based on evidence to illustrate the changes in the composition of the nucleus of the |
|The total number of neutrons plus protons does not change in any nuclear process. |atom and the energy released during the processes of fission, fusion, and radioactive decay. |
|In nuclear processes, atoms are not conserved, but the total number of protons plus neutrons is |Use simple qualitative models based on evidence to illustrate the scale of energy released in nuclear|
|conserved. |processes relative to other kinds of transformations. |
| |Develop models based on evidence to illustrate the changes in the composition of the nucleus of the |
| |atom and the energy released during the processes of alpha, beta, and gamma radioactive decays. |
|Part B: How do stars produce elements? |
|Concepts |Formative Assessment |
|The study of stars’ light spectra and brightness is used to identify compositional elements of stars,|Students who understand the concepts are able to: |
|their movements, and their distances from Earth. Other than the hydrogen and helium formed at the |Communicate scientific ideas in multiple formats (including orally, graphically, textually, and |
|time of the Big Bang, nuclear fusion within stars produces all atomic nuclei lighter than and |mathematically) about the way stars, over their life cycles, produce elements. |
|including iron, and the process releases electromagnetic energy. Heavier elements are produced when |Communicate scientific ideas about the way nucleosynthesis, and therefore the different elements it |
|certain massive stars achieve a supernova stage and explode. |creates, vary as a function of the mass of a star and the stage of its lifetime. |
|In nuclear processes, atoms are not conserved, but the total number of protons plus neutrons is |Communicate scientific ideas about how in nuclear processes, atoms are not conserved, but the total |
|conserved. |number of protons plus neutrons is conserved. |
|Part C: Is the life span of a star predictable? |
|Concepts |Formative Assessment |
|The star called the sun is changing and will burn out over a lifespan of approximately 10 billion |Students who understand the concepts are able to: |
|years. |Develop a model based on evidence to illustrate the life span of the sun and the role of nuclear |
|Nuclear fusion processes in the center of the sun release the energy that ultimately reaches Earth as|fusion in the sun's core in releasing energy that eventually reaches Earth in the form of radiation. |
|radiation. |Develop a model based on evidence to illustrate the relationships between nuclear fusion in the sun's|
|The significance of the energy transfer mechanisms that allow energy from nuclear fusion in the sun's|core and radiation that reaches Earth. |
|core to reach Earth is dependent on the scale, proportion, and quantity at which it occurs. | |
|Part D: If there was nobody there to Tweet about it, how do we know that there was a Big Bang? |
|Concepts |Formative Assessment |
|The study of stars’ light spectra and brightness is used to identify compositional elements of stars,|Students who understand the concepts are able to: |
|their movements, and their distances from Earth. |Construct an explanation of the Big Bang theory based on astronomical evidence of light spectra, |
|The Big Bang theory is supported by observations of distant galaxies receding from our own, of the |motion of distant galaxies, and composition of matter in the universe. |
|measured composition of stars and nonstellar gases, and of the maps of spectra of the primordial |Construct an explanation of the Big Bang theory based on the astronomical evidence of the red shift |
|radiation (cosmic microwave background) that still fills the universe. |of light from galaxies as an indication that the universe is currently expanding, the cosmic |
|Other than the hydrogen and helium formed at the time of the Big Bang, nuclear fusion within stars |microwave background as the remnant radiation from the Big Bang, and the observed composition of |
|produces all atomic nuclei lighter than and including iron, and the process releases electromagnetic |ordinary matter of the universe, primarily found in stars and interstellar gases (from the spectra of|
|energy. Heavier elements are produced when certain massive stars achieve a supernova stage and |electromagnetic radiation from stars). |
|explode. |Construct an explanation based on valid and reliable evidence that energy in the universe cannot be |
|Atoms of each element emit and absorb characteristic frequencies of light. These characteristics |created or destroyed, only moved between one place and another place, between objects and/or fields, |
|allow identification of the presence of an element, even in microscopic quantities. |or between systems. |
|Energy cannot be created or destroyed, only moved between one place and another place, between | |
|objects and/or fields, or between systems. | |
|Science and engineering complement each other in the cycle known as research and development (R&D). | |
|Many R&D projects may involve scientists, engineers, and others with wide ranges of expertise. | |
|Scientific knowledge is based on the assumption that natural laws operate today as they did in the | |
|past and will continue to do so in the future. | |
|Science assumes the universe is a vast single system in which basic laws are consistent. | |
|A scientific theory is a substantiated explanation of some aspect of the natural world, based on a | |
|body of facts that have been repeatedly confirmed through observation and experiment, and the science| |
|community validates each theory before it is accepted. If new evidence is discovered that the theory | |
|does not accommodate, the theory is generally modified in light of this new evidence. | |
|Part E: How can chemistry help us to figure out ancient events? |
|Concepts |Formative Assessment |
|Although active geologic processes, such as plate tectonics and erosion, have destroyed or altered |Students who understand the concepts are able to: |
|most of the very early rock record on Earth, other objects in the solar system, such as lunar rocks, |Apply scientific reasoning and evidence from ancient Earth materials, meteorites, and other planetary|
|asteroids, meteorites, have changed little over billions of years. Studying these objects can provide|surfaces to construct an account of Earth’s formation and early history. |
|information about Earth’s formation and early history. |Use available evidence within the solar system to reconstruct the early history of Earth, which |
|Spontaneous radioactive decays follow a characteristic exponential decay law. Nuclear lifetimes allow|formed along with the rest of the solar system 4.6 billion years ago. |
|radiometric dating to be used to determine the ages of rocks and other materials. |Apply scientific reasoning to link evidence from ancient Earth materials, meteorites, and other |
|Much of science deals with constructing explanations of how things change and how they remain stable.|planetary surfaces to claims about Earth’s formation and early history, and assess the extent to |
| |which the reasoning and data support the explanation or conclusion. |
| |Use available evidence within the solar system to construct explanations for how Earth has changed |
| |and how it remains stable. |
|What It Looks Like in the Classroom |
|This unit of study explores the flow of energy and matter but with emphasis on Earth and space science in relation to the history of Earth starting with the Big Bang theory. Students explore the |
|production of elements in stars and radioactive decay. Students develop and use models to illustrate the processes of fission, fusion, and radioactive decay and the scale of energy released in nuclear |
|processes. Models are qualitative, based on evidence, and might include depictions of radioactive decay series such as Uranium-238, chain reactions such as the fission of Uranium-235 in reactors, and |
|fusion within the core of stars. Students also explore the PhET nuclear fission inquiry lab and graphs to illustrate the changes in the composition of the nucleus of the atom and the energy released |
|during the processes of alpha, beta, and gamma radioactive decays. When modeling nuclear processes, students depict that atoms are not conserved, but the total number of protons plus neutrons is |
|conserved. Models include changes in the composition of the nucleus of atoms and the scale of energy released in nuclear processes. |
|The study of stars’ light spectra and brightness is used to identify compositional elements of stars, their movements, and their distances from Earth. Other than hydrogen and helium formed at the time of|
|the Big Bang, nuclear fusion within stars produces all atomic nuclei lighter than and including iron, and the process releases electromagnetic energy. Heavier elements are produced when certain massive |
|stars achieve a supernova stage and explode. Because atoms of each element emit and absorb characteristic frequencies of light, the presence of an element can be detected in stars and interstellar gases.|
|Students develop an understanding of how analysis of light spectra gives us information about the composition of stars and interstellar gases. Communication of scientific ideas about how stars produce |
|elements is done in multiple formats, including orally, graphically, textually, and mathematically. The conservation of the total number of protons plus neutrons is important in their explanations, and |
|students should cite supporting evidence from text. |
|Students use the sun as a model for the lifecycle of a star. This model should also illustrate the relationship between nuclear fusion in the sun’s core and energy that reaches the Earth in the form of |
|radiation. Students construct a mathematical model of nuclear fusion in the sun’s core, identifying important quantities and factors that affect the life span of the sun. They use units and consider |
|limitations on measurement when describing energy from nuclear fusion in the sun’s core that reaches the Earth. For example, students quantify the amounts of energy in joules when comparing energy |
|sources. In this way, students develop an understanding of how our sun changes and how it will burn out over a lifespan of approximately 10 billion years. |
|This unit continues with a study of how astronomical evidence (“red shift/blue shift,” wavelength relationships to energy, and universe expansion) can be used to support the Big Bang theory. Students |
|construct an explanation of the Big Bang theory based on evidence of light spectra, motion of distant galaxies, and composition of matter in the universe. Students explore and cite evidence from text of |
|distant galaxies receding from our own, of the measured composition of stars and nonstellar gases, and of the maps of spectra of primordial radiation that still fills the universe. The concept of |
|conservation of energy should be evident in student explanations. Students cite specific evidence from text to support their explanations of the life cycle of stars, the role of nuclear fusion in the |
|sun’s core, and the Big Bang theory. In their explanations, they discuss the idea that science assumes the universe is a vast single system in which laws are consistent. |
|Students are aware that a scientific theory is a substantiated explanation of some aspect of the natural world, based on a body of facts that have been repeatedly confirmed through observation and |
|experiment, and the science community validates each theory before it is accepted. Students know that if new evidence is discovered that the theory does not accommodate, the theory is generally modified |
|in light of the new evidence. |
|This unit concludes with the application of scientific reasoning and the use of evidence from ancient Earth materials, meteorites, and other planetary surfaces to construct an account of the Earth’s |
|formation and early history. For example, students use examples of spontaneous radioactive decay as a tool to determine the ages of rocks or other materials (K-39 to Ar-40). Students make claims about |
|Earth’s formation and early history supported by data while considering appropriate units, quantities and limitations on measurement. Students construct graphs showing data on the absolute ages and |
|composition of Earth’s rocks, lunar rocks, and meteorites. Using available evidence within the solar system, students construct explanations for how the earth has changed and how it has remained stable |
|in its 4.6 billion year history. |
|Connecting with English Language Arts/Literacy and Mathematics |
|English Language Arts/Literacy |
|Ask and refine questions to support uniform energy distribution among the components in a system when two components of different temperature are combined, using specific textual evidence. |
|Conduct short as well as more sustained research projects to determine energy distribution in a system when two components of different temperature are combined. |
|Collect relevant data across a broad spectrum of sources about the distribution of energy in a system and assess the strengths and limitations of each source. |
|Synthesize findings from experimental data into a coherent understanding of energy distribution in a system. |
|Conduct short as well as more sustained research projects to determine how the properties of water affect Earth materials and surface processes. |
|Cite specific textual evidence to evaluate competing design solutions for developing, managing, and utilizing energy and mineral resources based on cost–benefit ratios. |
|Evaluate the hypotheses, data, analysis, and conclusions of competing design solutions for developing, managing, and utilizing energy and mineral resources based on cost–benefit ratios, verifying the |
|data when possible and corroborating or challenging conclusions with other design solutions. |
|Integrate and evaluate multiple design solutions for developing, managing, and utilizing energy and mineral resources based on cost–benefit ratios in order to reveal meaningful patterns and trends. |
|Evaluate the hypotheses, data, analysis, and conclusions of competing design solutions for developing, managing, and utilizing energy and mineral resources based on cost–benefit ratios, verifying the |
|data when possible and corroborating or challenging conclusions with other design solutions. |
|Synthesize data from multiple sources of information in order to create data sets that inform design decisions and create a coherent understanding of developing, managing, and utilizing energy and |
|mineral resources. |
|Mathematics |
|Use symbols to represent energy distribution in a system when two components of different temperature are combined, and manipulate the representing symbols. Make sense of quantities and relationships in |
|the energy distribution in a system when two components of different temperature are combined. |
|Use a mathematical model to describe energy distribution in a system when two components of different temperature are combined. Identify important quantities in energy distribution in a system when two |
|components of different temperature are combined and map their relationships using tools. Analyze those relationships mathematically to draw conclusions, reflecting on the results and improving the model|
|if it has not served its purpose. |
|Choose a level of accuracy appropriate to limitations on measurement when reporting quantities of the properties of water and their effects on Earth materials and surface processes. |
|Use symbols to represent an explanation of the best of multiple design solutions for developing, managing, and utilizing energy and mineral resources and manipulate the representing symbols. Make sense |
|of quantities and relationships in cost–benefit ratios for multiple design solutions for developing, managing, and utilizing energy and mineral resources symbolically and manipulate the representing |
|symbols. |
|Use a mathematical model to explain the evaluation of multiple design solutions for developing, managing, and utilizing energy and mineral resources. Identify important quantities in cost–benefit ratios |
|for multiple design solutions for developing, managing, and utilizing energy and mineral resources and map their relationships using tools. Analyze those relationships mathematically to draw conclusions,|
|reflecting on the results and improving the model if it has not served its purpose. |
|Modifications |
|(Note: Teachers identify the modifications that they will use in the unit. See NGSS Appendix D: All Standards, All Students/Case Studies for vignettes and explanations of the modifications.) |
|Structure lessons around questions that are authentic, relate to students’ interests, social/family background and knowledge of their community. |
|Provide students with multiple choices for how they can represent their understandings (e.g. multisensory techniques-auditory/visual aids; pictures, illustrations, graphs, charts, data tables, |
|multimedia, modeling). |
|Provide opportunities for students to connect with people of similar backgrounds (e.g. conversations via digital tool such as SKYPE, experts from the community helping with a project, journal articles, |
|and biographies). |
|Provide multiple grouping opportunities for students to share their ideas and to encourage work among various backgrounds and cultures (e.g. multiple representation and multimodal experiences). |
|Engage students with a variety of Science and Engineering practices to provide students with multiple entry points and multiple ways to demonstrate their understandings. |
|Use project-based science learning to connect science with observable phenomena. |
|Structure the learning around explaining or solving a social or community-based issue. |
|Provide ELL students with multiple literacy strategies. |
|Collaborate with after-school programs or clubs to extend learning opportunities. |
|Restructure lesson using UDL principals (). |
|Research on Student Learning |
|Students of all ages show a wide range of beliefs about the nature and behavior or particles. They lack an appreciation of the very small size of particles; believe there must be something in the space |
|between particles; have difficulty in appreciating the intrinsic motion of particles in solids, liquids and gases; and have problems in conceptualizing forces between particles (NSDL, 2015). |
|Prior Learning |
|Physical science |
|Substances are made from different types of atoms, which combine with one another in various ways. Atoms form molecules that range in size from two to thousands of atoms. |
|Each pure substance has characteristic physical and chemical properties (for any bulk quantity under given conditions) that can be used to identify it. |
|Gases and liquids are made of molecules or inert atoms that are moving about relative to each other. |
|In a liquid, the molecules are constantly in contact with others; in a gas, they are widely spaced except when they happen to collide. In a solid, atoms are closely spaced and may vibrate in position but|
|do not change relative locations. |
|Solids may be formed from molecules, or they may be extended structures with repeating subunits (e.g., crystals). |
|The changes of state that occur with variations in temperature or pressure can be described and predicted using these models of matter. |
|Substances react chemically in characteristic ways. In a chemical process, the atoms that make up the original substances are regrouped into different molecules, and these new substances have different |
|properties from those of the reactants. |
|The total number of each type of atom is conserved, and thus the mass does not change. |
|Some chemical reactions release energy, others store energy. |
|When light shines on an object, it is reflected, absorbed, or transmitted through the object, depending on the object’s material and the frequency (color) of the light. |
|The path that light travels can be traced as straight lines, except at surfaces between different transparent materials (e.g., air and water, air and glass) where the light path bends. |
|A wave model of light is useful for explaining brightness, color, and the frequency-dependent bending of light at a surface between media. |
|However, because light can travel through space, it cannot be a matter wave, like sound or water waves. |
|Earth and space science |
|Patterns of the apparent motion of the sun, the moon, and stars in the sky can be observed, described, predicted, and explained with models. |
|Earth and its solar system are part of the Milky Way Galaxy, which is one of many galaxies in the universe. |
|All Earth processes are the result of energy flowing and matter cycling within and among the planet’s systems. This energy is derived from the sun and Earth’s hot interior. The energy that flows and |
|matter that cycles produce chemical and physical changes in Earth’s materials and living organisms. |
|The planet’s systems interact over scales that range from microscopic to global in size, and they operate over fractions of a second to billions of years. These interactions have shaped Earth’s history |
|and will determine its future. |
|Connections to other Courses |
|Physical science |
|Each atom has a charged substructure consisting of a nucleus, which is made of protons and neutrons, surrounded by electrons. |
|The periodic table orders elements horizontally by the number of protons in the atom’s nucleus and places elements with similar chemical properties in columns. The repeating patterns of this table |
|reflect patterns of outer electron states. |
|The structure and interactions of matter at the bulk scale are determined by electrical forces within and between atoms. |
|A stable molecule has less energy than the same set of atoms separated; one must provide at least this energy in order to take the molecule apart. |
|Nuclear processes, including fusion, fission, and radioactive decays of unstable nuclei, involve release or absorption of energy. The total number of neutrons plus protons does not change in any nuclear |
|process. |
|Energy is a quantitative property of a system that depends on the motion and interactions of matter and radiation within that system. That there is a single quantity called energy is due to the fact that|
|a system’s total energy is conserved, even as, within the system, energy is continually transferred from one object to another and between its various possible forms. |
|Conservation of energy means that the total change of energy in any system is always equal to the total energy transferred into or out of the system. |
|Energy cannot be created or destroyed, but it can be transported from one place to another and transferred between systems. |
|Mathematical expressions, which quantify how the stored energy in a system depends on its configuration (e.g., relative positions of charged particles, compression of a spring) and how kinetic energy |
|depends on mass and speed, allow the concept of conservation of energy to be used to predict and describe system behavior. |
|The availability of energy limits what can occur in any system. |
|Uncontrolled systems always evolve toward more stable states—that is, toward more uniform energy distribution (e.g., water flows downhill, objects hotter than their surrounding environment cool down). |
|When two objects interacting through a field change relative position, the energy stored in the field is changed. |
|Although energy cannot be destroyed, it can be converted to less useful forms—for example, to thermal energy in the surrounding environment. |
|Electromagnetic radiation (e.g., radio, microwaves, light) can be modeled as a wave of changing electric and magnetic fields or as particles called photons. The wave model is useful for explaining many |
|features of electromagnetic radiation, and the particle model explains other features. |
|When light or longer wavelength electromagnetic radiation is absorbed in matter, it is generally converted into thermal energy (heat). Shorter wavelength electromagnetic radiation (ultraviolet, X-rays, |
|gamma rays) can ionize atoms and cause damage to living cells. |
|Photoelectric materials emit electrons when they absorb light of a high-enough frequency. |
|Earth and space science |
|The star called the sun is changing and will burn out over a lifespan of approximately 10 billion years. |
|The study of stars’ light spectra and brightness is used to identify compositional elements of stars, their movements, and their distances from Earth. |
|The Big Bang theory is supported by observations of distant galaxies receding from our own, of the measured composition of stars and nonstellar gases, and of the maps of spectra of the primordial |
|radiation (cosmic microwave background) that still fills the universe. |
|Other than the hydrogen and helium formed at the time of the Big Bang, nuclear fusion within stars produces all atomic nuclei lighter than and including iron, and the process releases electromagnetic |
|energy. Heavier elements are produced when certain massive stars achieve a supernova stage and explode. |
|Continental rocks, which can be older than 4 billion years, are generally much older than the rocks of the ocean floor, which are less than 200 million years old. |
|Although active geologic processes, such as plate tectonics and erosion, have destroyed or altered most of the very early rock record on Earth, other objects in the solar system, such as lunar rocks, |
|asteroids, and meteorites, have changed little over billions of years. Studying these objects can provide information about Earth’s formation and early history. |
|Sample of Open Education Resources |
|Solar Fusion: Students develop a model to identify and describe the hydrogen as the Sun’s fuel source, helium and energy as the products of nuclear fusion, and the life span of the Sun. |
|Expansion of the Universe & Four Pillars of Cosmology: Student analyze informational text, animations and videos on the Doppler effect and the observed redshift in the universe. Students apply their |
|learning of the Doppler effect to justify the Big Bang Theory and support their reasoning with evidence from multiple sources. |
|Extensions: |
|Sonic Boom Link: |
|Echolocation Link: |
|Universe Evolution & CMB Analyzer: Students analyze several NASA concept animations to develop an explanation for the existence of background radiation and the redshift to defend the argument that the |
|universe is expanding. |
|Life Cycle of a Star - Students analyze multiple sources of information text and diagrams on the life cycle of a star. Students use the text to determine the relationship between the stars’ mass, life |
|cycle and ability to fuse elements and ability to go spread the elements through the universe. |
|Emission Spectrum of the Sun - Students analyze informational text and a video on how scientists know the composition of the sun. Students use the information to develop a written argument on how |
|scientists can use this method to determine the composition of distant stars. |
|Interactive HR Diagram - Students manipulate the variables of the HR diagram to determine the relationship between the mass, lifespan, color and size of a star. Students generate conclusion between the |
|mass and the lifespan of the star supported with data from the activity. |
|Supernova - Students analyze informational text regarding supernova to determine where a supernova takes place, the cause of supernovas and the role of supernovas in the evolution of the universe. |
|Appendix A: NGSS and Foundations for the Unit |
|Develop models to illustrate the changes in the composition of the nucleus of the atom and the energy released during the processes of fission, fusion, and radioactive decay. [Clarification Statement: |
|Emphasis is on simple qualitative models, such as pictures or diagrams, and on the scale of energy released in nuclear processes relative to other kinds of transformations.] [Assessment Boundary: |
|Assessment does not include quantitative calculation of energy released. Assessment is limited to alpha, beta, and gamma radioactive decays.] (HS-PS1-8) |
|Communicate scientific ideas about the way stars, over their life cycle, produce elements. [Clarification Statement: Emphasis is on the way nucleosynthesis, and therefore the different elements created, |
|varies as a function of the mass of a star and the stage of its lifetime.] [Assessment Boundary: Details of the many different nucleosynthesis pathways for stars of differing masses are not assessed.] |
|(HS-ESS1-3) |
|Develop a model based on evidence to illustrate the life span of the sun and the role of nuclear fusion in the sun’s core to release energy that eventually reaches Earth in the form of radiation. |
|[Clarification Statement: Emphasis is on the energy transfer mechanisms that allow energy from nuclear fusion in the sun’s core to reach Earth. Examples of evidence for the model include observations of |
|the masses and lifetimes of other stars, as well as the ways that the sun’s radiation varies due to sudden solar flares (“space weather”), the 11-year sunspot cycle, and non-cyclic variations over |
|centuries.] [Assessment Boundary: Assessment does not include details of the atomic and subatomic processes involved with the sun’s nuclear fusion.] (HS-ESS1-1) |
|Construct an explanation of the Big Bang theory based on astronomical evidence of light spectra, motion of distant galaxies, and composition of matter in the universe. [Clarification Statement: Emphasis |
|is on the astronomical evidence of the red shift of light from galaxies as an indication that the universe is currently expanding, the cosmic microwave background as the remnant radiation from the Big |
|Bang, and the observed composition of ordinary matter of the universe, primarily found in stars and interstellar gases (from the spectra of electromagnetic radiation from stars), which matches that |
|predicted by the Big Bang theory (3/4 hydrogen and 1/4 helium).] (HS-ESS1-2) |
|Apply scientific reasoning and evidence from ancient Earth materials, meteorites, and other planetary surfaces to construct an account of Earth’s formation and early history. [Clarification Statement: |
|Emphasis is on using available evidence within the solar system to reconstruct the early history of Earth, which formed along with the rest of the solar system 4.6 billion years ago. Examples of evidence|
|include the absolute ages of ancient materials (obtained by radiometric dating of meteorites, moon rocks, and Earth’s oldest minerals), the sizes and compositions of solar system objects, and the impact |
|cratering record of planetary surfaces.] (HS-ESS1-6) |
|The Student Learning Objectives above were developed using the following elements from the NRC document A Framework for K-12 Science Education: |
|Science and Engineering Practices |Disciplinary Core Ideas |Crosscutting Concepts |
|Developing and Using Models |PS1.C: Nuclear Processes |Energy and Matter |
|Modeling in 9–12 builds on K–8 and progresses to using, |Nuclear processes, including fusion, fission, and radioactive |In nuclear processes, atoms are not conserved, but the total number|
|synthesizing, and developing models to predict and show |decays of unstable nuclei, involve release or absorption of energy.|of protons plus neutrons is conserved. (HS-ESS1-3), (HS-PS1-8), |
|relationships among variables between systems and their components |The total number of neutrons plus protons does not change in any |(HS-ESS1-1) |
|in the natural and designed worlds. |nuclear process. (HS-PS1-8) |Energy cannot be created or destroyed–only moved between one place |
|Develop a model based on evidence to illustrate the relationships |ESS1.A: The Universe and Its Stars |and another place, between objects and/or fields, or between |
|between systems or between components of a system. |The star called the sun is changing and will burn out over a |systems. (HS-ESS1-2) |
|(HS-PS1-8),(HS-ESS1-1) |lifespan of approximately 10 billion years. (HS-ESS1-1) |Scale, Proportion, and Quantity |
|Constructing Explanations and Designing Solutions |The study of stars’ light spectra and brightness is used to |The significance of a phenomenon is dependent on the scale, |
|Constructing explanations and designing solutions in 9–12 builds on|identify compositional elements of stars, their movements, and |proportion, and quantity at which it occurs. (HS-ESS1-1) |
|K–8 experiences and progresses to explanations and designs that are|their distances from Earth. (HS-ESS1-2),(HS-ESS1-3) |Algebraic thinking is used to examine scientific data and predict |
|supported by multiple and independent student-generated sources of |The Big Bang theory is supported by observations of distant |the effect of a change in one variable on another (e.g., linear |
|evidence consistent with scientific ideas, principles, and |galaxies receding from our own, of the measured composition of |growth vs. exponential growth). (HS-ESS1-4) |
|theories. |stars and non-stellar gases, and of the maps of spectra of the |In nuclear processes, atoms are not conserved, but the total number|
|Construct an explanation based on valid and reliable evidence |primordial radiation (cosmic microwave background) that still fills|of protons plus neutrons is conserved. (HS-PS1-8) |
|obtained from a variety of sources (including students’ own |the universe. (HS-ESS1-2) |Stability and Change |
|investigations, theories, simulations, peer review) and the |Other than the hydrogen and helium formed at the time of the Big |Much of science deals with constructing explanations of how things |
|assumption that theories and laws that describe the natural world |Bang, nuclear fusion within stars produces all atomic nuclei |change and how they remain stable. (HS-ESS1-6) |
|operate today as they did in the past and will continue to do so in|lighter than and including iron, and the process releases | - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - |
|the future. (HS-ESS1-2) |electromagnetic energy. Heavier elements are produced when certain |Connections to Engineering, Technology, and Applications of Science|
|Apply scientific reasoning to link evidence to the claims to assess|massive stars achieve a supernova stage and explode. |Interdependence of Science, Engineering, and Technology |
|the extent to which the reasoning and data support the explanation |(HS-ESS1-2),(HS-ESS1-3) |Science and engineering complement each other in the cycle known as|
|or conclusion. (HS-ESS1-6) |ESS1.C: The History of Planet Earth |research and development (R&D). Many R&D projects may involve |
|Obtaining, Evaluating, and Communicating Information |Although active geologic processes, such as plate tectonics and |scientists, engineers, and others with wide ranges of expertise. |
|Communicate scientific ideas (e.g. about phenomena and/or the |erosion, have destroyed or altered most of the very early rock |(HS-ESS1-2) |
|process of development and the design and performance of a proposed|record on Earth, other objects in the solar system, such as lunar |- -- - - - - - - - - - - - - - - - - - - - - - - - - - - - - - |
|process or system) in multiple formats (including orally, |rocks, asteroids, and meteorites, have changed little over billions| Connections to Nature of Science |
|graphically, textually, and mathematically). (HS-ESS1-3) |of years. Studying these objects can provide information about | Scientific Knowledge Assumes an Order and Consistency in Natural |
|Obtaining, evaluating, and communicating information in 9–12 builds|Earth’s formation and early history. (HS-ESS1-6) |Systems |
|on K–8 experiences and progresses to evaluating the validity and |PS3.D: Energy in Chemical Processes and Everyday Life |Scientific knowledge is based on the assumption that natural laws |
|reliability of the claims, methods, and designs. (HS-ESS1-6) |Nuclear Fusion processes in the center of the sun release the |operate today as they did in the past and they will continue to do |
| |energy that ultimately reaches Earth as radiation. (secondary) |so in the future. (HS-ESS1-2) |
| |(HS-ESS1-1) |Science assumes the universe is a vast single system in which basic|
| |PS4.B: Electromagnetic Radiation |laws are consistent. (HS-ESS1-2) |
| |Atoms of each element emit and absorb characteristic frequencies of|Science Models, Laws, Mechanisms, and Theories Explain Natural |
| |light. These characteristics allow identification of the presence |Phenomena |
| |of an element, even in microscopic quantities.(secondary)HS-ESS1-2)|A scientific theory is a substantiated explanation of some aspect |
| | |of the natural world, based on a body of facts that have been |
| | |repeatedly confirmed through observation and experiment and the |
| | |science community validates each theory before it is accepted. If |
| | |new evidence is discovered that the theory does not accommodate, |
| | |the theory is generally modified in light of this new evidence. |
| | |(HS-ESS1-2) |
|English Language Arts/Literacy |Mathematics |
|Cite specific textual evidence to support analysis of science and technical texts, attending to |Reason abstractly and quantitatively. (HS-ESS1-1), (HS-ESS1-2) ,(HS-ESS1-3) , (HS-ESS1-6) MP.2 |
|important distinctions the author makes and to any gaps or inconsistencies in the |Model with mathematics. (HS-ESS1-1), (HS-PS1-8), (HS-ESS1-6) MP.4 |
|account. (HS-ESS1-1) RST.11-12.1 |Use units as a way to understand problems and to guide the solution of multi-step problems; choose |
|Evaluate the hypotheses, data, analysis, and conclusions in a science or technical text, verifying |and interpret units consistently in formulas; choose and interpret the scale and the origin in graphs|
|the data when possible and corroborating or challenging conclusions with other sources of |and data displays. (HS-ESS1-1),(HS-ESS1-2), (HS-PS1-8), (HS-ESS1-6) HSN-Q.A.1 |
|information. (HS-ESS1-6) RST.11-12.8 |Define appropriate quantities for the purpose of descriptive modeling. (HS-ESS1-1), (HS-ESS1-2), |
|Write informative/explanatory texts, including the narration of historical events, scientific |(HS-PS1-8), (HS-ESS1-6) HSN-Q.A.2 |
|procedures/ experiments, or technical processes. (HS-ESS1-3),(HS-ESS1-2) WHST.9-12.2 |Choose a level of accuracy appropriate to limitations on measurement when reporting |
|Write arguments focused on discipline-specific content. (HS-ESS1-6) WHST.9-12.1 |quantities. (HS-ESS1-1), (HS-ESS1-2), (HS-PS1-8), (HS-ESS1-6) HSN-Q.A.3 |
|Present claims and findings, emphasizing salient points in a focused, coherent manner with relevant |Interpret expressions that represent a quantity in terms of its context. (HS-ESS1-1) HSA-SSE.A.1 |
|evidence, sound valid reasoning, and well-chosen details; use appropriate eye contact, adequate |Create equations in two or more variables to represent relationships between quantities; graph |
|volume, and clear pronunciation. (HS-ESS1-3) SL.11-12.4 |equations on coordinate axes with labels and scales. (HS-ESS1-1), (HS-ESS1-2) HSA-CED.A.2 |
| |Rearrange formulas to highlight a quantity of interest, using the same reasoning as in solving |
| |equations. (HS-ESS1-1),(HS-ESS1-2) HSA-CED.A.4 |
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